From 96190371963a04d7a0381a17f6dd8f6fe949cae0 Mon Sep 17 00:00:00 2001 From: Alex Drlica-Wagner Date: Tue, 29 Jan 2019 23:04:05 -0600 Subject: [PATCH] direct --- complement/direct.tex | 4 +- main.bib | 88 ++++++++++++++++++++++++++++--------------- 2 files changed, 59 insertions(+), 33 deletions(-) diff --git a/complement/direct.tex b/complement/direct.tex index b40e6de..582bd3c 100644 --- a/complement/direct.tex +++ b/complement/direct.tex @@ -24,11 +24,11 @@ \subsection{Local Dark Matter Distribution \Contact{Lina}} \end{equation} where $\sigma_\chi$ and $m_\chi$ are the interaction cross section and mass of the dark matter particle, $|F(E)|$ is a nuclear form factor that depends on the choice of detector material, $m_N$ is the mass of the target nucleus, $\mu$ is the reduced mass of the dark matter-nucleus system, $v = |{\bf v}|$ is the speed of the dark matter particles, $f({\bf v},t)$ is the velocity distribution function of the dark matter particles, $v_\mathrm{max} = 533^{+54}_{-41}\kms$ (at 90\% confidence) is the Galactic escape speed \citep{2014AA...562A..91P}; and $\rhodmlab$ is the dark matter density within the detector. -From equation \ref{eqn:recoilrate}, we can see that $\rhodmlab$ trivially degenerates with the properties of the dark matter particle, $\sigma_W/m_W$. For this reason, significant effort has gone into estimating the amount of dark matter within a few hundred parsecs of the Sun, $\rhodm$, from which we can extrapolate $\rhodmlab$ \citep[see][for a review]{2014JPhG...41f3101R}. The latest values favor $\rhodm \sim 0.5\,{\rm GeV cm}^{-3}$, with an uncertainty of order $20-30$\% \citep[\eg,][]{2014A&A...571A..92B,2018MNRAS.478.1677S}. With the advent of unprecedented data from the \Gaia satellite, the systematic and random errors on $\rhodm$ will continue to fall \citep{2014JPhG...41f3101R}. However, equally important in equation \ref{eqn:recoilrate} is the velocity distribution function of dark matter, $f({\bf v},t)$, which is much more challenging to measure.\footnote{The time dependence of $f({\bf v},t)$ owes primarily to the motion of the Earth around the Sun and is, therefore, straightforward to calculate \citep[\eg,][]{1986PhRvD..33.3495D}.} +From equation \ref{eqn:recoilrate}, we can see that $\rhodmlab$ trivially degenerates with the properties of the dark matter particle, $\sigma_\chi/m_\chi$. For this reason, significant effort has gone into estimating the amount of dark matter within a few hundred parsecs of the Sun, $\rhodm$, from which we can extrapolate $\rhodmlab$ \citep[see][for a review]{2014JPhG...41f3101R}. The latest values favor $\rhodm \sim 0.5\,{\rm GeV cm}^{-3}$, with an uncertainty of order $20-30$\% \citep[\eg,][]{2014A&A...571A..92B,2018MNRAS.478.1677S}. With the advent of unprecedented data from the \Gaia satellite, the systematic and random errors on $\rhodm$ will continue to fall \citep{2014JPhG...41f3101R}. However, equally important in equation \ref{eqn:recoilrate} is the velocity distribution function of dark matter, $f({\bf v},t)$, which is much more challenging to measure.\footnote{The time dependence of $f({\bf v},t)$ owes primarily to the motion of the Earth around the Sun and is, therefore, straightforward to calculate \citep[\eg,][]{1986PhRvD..33.3495D}.} The shape of $f({\bf v})$ has been constrained primarily by numerical simulations of structure formation in the standard cosmological model \citep[\eg,][]{2009MNRAS.395..797V,1210.2721}. Such simulations include treatments to model the effects of unresolved substructure and debris, and the impact of dark matter particles scattering within the solar system \citep[\eg,][]{2009PhRvD..79j3531P}. However, such effects can only be treated statistically and might not apply to the real $f({\bf v})$ in our Galaxy. -With the advent of LSST, we will be able to {\it empirically} probe $f({\bf v})$ with unprecedented precision. The key idea is to use the oldest and most metal poor stars, which were accreted onto the Milky Way as it formed, as luminous tracers of the underlying dark matter halo \citep{Lisanti:2011as,Kuhlen:2012fz,2014MNRAS.445L..21T,Lisanti:2014dva,2018PhRvL.120d1102H}. Such accreted stars also trace the presence of a `dark disk' formed from the late accretion of massive and more metal rich satellites \citep{1989AJ.....98.1554L,2008MNRAS.389.1041R,2009MNRAS.397...44R,2014MNRAS.444..515R,2015MNRAS.450.2874R}, and structures that are not yet fully phase mixed like `debris flows' \citep[\eg,][]{Lisanti:2011as}, tidal streams \citep[\eg,][]{2005PhRvD..71d3516F}, and more major mergers \citep{2018MNRAS.477.1472B,2018Natur.563...85H,necib2018}. All of these structures imprint features on $f({\bf v})$ that alter the expected flux at a given recoil energy in dark matter detection experiments, and the expected annual modulation signal \citep[\eg,][]{2005PhRvD..71d3516F,2009ApJ...696..920B,2018arXiv181011468E}. +With the advent of LSST, we will be able to {\it empirically} probe $f({\bf v})$ with unprecedented precision. The key idea is to use the oldest and most metal poor stars, which were accreted onto the Milky Way as it formed, as luminous tracers of the underlying dark matter halo \citep{Lisanti:2011as,Kuhlen:2012fz,2014MNRAS.445L..21T,Lisanti:2014dva,2018PhRvL.120d1102H,Necib:2018b}. Such accreted stars also trace the presence of a `dark disk' formed from the late accretion of massive and more metal rich satellites \citep{1989AJ.....98.1554L,2008MNRAS.389.1041R,2009MNRAS.397...44R,2014MNRAS.444..515R,2015MNRAS.450.2874R}, and structures that are not yet fully phase mixed like `debris flows' \citep[\eg,][]{Lisanti:2011as,2018MNRAS.477.1472B,2018Natur.563...85H,necib2018} and tidal streams \citep[\eg,][]{2005PhRvD..71d3516F,1807.09004}. All of these structures imprint features on $f({\bf v})$ that alter the expected flux at a given recoil energy in dark matter detection experiments, and the expected annual modulation signal \citep[\eg,][]{2005PhRvD..71d3516F,2009ApJ...696..920B,2018arXiv181011468E}. The wide sky coverage and depth of LSST will allow us to select metal poor halo star candidates in statistically significant quantities \citep[\eg,][]{2017MNRAS.471.2587S}, with proper motion data available for the brighter stars. Combined with follow up spectroscopy, this will provide a direct probe of the velocity distribution of the Milky Way's smooth phase mixed component \citep{2018PhRvL.120d1102H}. In addition, LSST will find a slew of new structures and streams, allowing us to probe also the non-phased mixed component \citep{2005PhRvD..71d3516F,2018arXiv181011468E}. Finally, combining LSST with spectroscopic surveys of the disk will allow us to place ever tighter constraints on the possible presence of a dark disk \citep{2015MNRAS.450.2874R}. diff --git a/main.bib b/main.bib index 8839c24..a84c44c 100644 --- a/main.bib +++ b/main.bib @@ -1119,18 +1119,45 @@ @article{Goodman:1984dc SLACcitation = "%%CITATION = PHRVA,D31,3059;%%" } -@article{necib2018, - Archiveprefix = {arXiv}, - Author = {Necib, Lina and Lisanti, Mariangela and Belokurov, Vasily}, - Date-Added = {2018-07-20 02:36:18 +0000}, - Date-Modified = {2018-08-01 18:34:17 -0700}, - Eprint = {1807.02519}, - Journal = {Submitted to ApJ}, - Primaryclass = {astro-ph.GA}, - Slaccitation = {%%CITATION = ARXIV:1807.02519;%%}, - Title = {{Dark Matter in Disequilibrium: The Local Velocity Distribution from SDSS-Gaia}}, - Year = {2018}} +@ARTICLE{necib2018, + author = {{Necib}, Lina and {Lisanti}, Mariangela and {Belokurov}, Vasily}, + title = "{Dark Matter in Disequilibrium: The Local Velocity Distribution from SDSS-Gaia}", + journal = {arXiv e-prints}, + keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology}, + year = 2018, + month = Jul, + eid = {arXiv:1807.02519}, + pages = {arXiv:1807.02519}, +archivePrefix = {arXiv}, + eprint = {1807.02519}, + primaryClass = {astro-ph.GA}, + adsurl = {https://ui.adsabs.harvard.edu/\#abs/2018arXiv180702519N}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} + + +@ARTICLE{Necib:2018b, + author = {{Necib}, Lina and {Lisanti}, Mariangela and {Garrison-Kimmel}, Shea and + {Wetzel}, Andrew and {Sanderson}, Robyn and {Hopkins}, Philip F. + and {Faucher-Gigu{\`e}re}, Claude-Andr{\'e} and {Kere{\v{s}}}, + Du{\v{s}}an}, + title = "{Under the Firelight: Stellar Tracers of the Local Dark Matter Velocity + Distribution in the Milky Way}", + journal = {ArXiv e-prints}, + keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and + Nongalactic Astrophysics, High Energy Physics - Phenomenology}, + year = 2018, + month = Oct, + eid = {arXiv:1810.12301}, + pages = {arXiv:1810.12301}, +archivePrefix = {arXiv}, + eprint = {1810.12301}, + primaryClass = {astro-ph.GA}, + adsurl = {https://ui.adsabs.harvard.edu/#abs/2018arXiv181012301N}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} + @article{Herzog-Arbeitman:2017zbm, Archiveprefix = {arXiv}, Author = {Herzog-Arbeitman, Jonah and Lisanti, Mariangela and Necib, Lina}, @@ -1185,26 +1212,6 @@ @ARTICLE{2018MNRAS.475.1537M -@ARTICLE{Necib:2018b, - author = {{Necib}, Lina and {Lisanti}, Mariangela and {Garrison-Kimmel}, Shea and - {Wetzel}, Andrew and {Sanderson}, Robyn and {Hopkins}, Philip F. - and {Faucher-Gigu{\`e}re}, Claude-Andr{\'e} and {Kere{\v{s}}}, - Du{\v{s}}an}, - title = "{Under the Firelight: Stellar Tracers of the Local Dark Matter Velocity - Distribution in the Milky Way}", - journal = {ArXiv e-prints}, - keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and - Nongalactic Astrophysics, High Energy Physics - Phenomenology}, - year = 2018, - month = Oct, - eid = {arXiv:1810.12301}, - pages = {arXiv:1810.12301}, -archivePrefix = {arXiv}, - eprint = {1810.12301}, - primaryClass = {astro-ph.GA}, - adsurl = {https://ui.adsabs.harvard.edu/#abs/2018arXiv181012301N}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} @@ -11837,3 +11844,22 @@ @article{2018PhRvL.120d1102H year = {2018} } +@ARTICLE{1807.09004, + author = {{O'Hare}, Ciaran A.~J. and {McCabe}, Christopher and {Evans}, N. Wyn and + {Myeong}, GyuChul and {Belokurov}, Vasily}, + title = "{Dark matter hurricane: Measuring the S1 stream with dark matter detectors}", + journal = {\prd}, + keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Experiment, High Energy Physics - Phenomenology}, + year = 2018, + month = Nov, + volume = {98}, + eid = {103006}, + pages = {103006}, + doi = {10.1103/PhysRevD.98.103006}, +archivePrefix = {arXiv}, + eprint = {1807.09004}, + primaryClass = {astro-ph.CO}, + adsurl = {https://ui.adsabs.harvard.edu/\#abs/2018PhRvD..98j3006O}, + adsnote = {Provided by the SAO/NASA Astrophysics Data System} +} +